In non-outbursting low-mass YSO (T Tauri stars) the mass-infall is believed to proceed through magnetospheric accretion columns operating between the inner disk and the photosphere [1]}. It is not yet understood how the accretion geometry differs in highly-accreting FUors, which also limits our understanding of the outburst-triggering mechanisms. In order to further our understanding of these processes we have conducted the first tri-waveband NIR interferometric study of a YSO at the CHARA array using MIRC-X in the J and H bands. These include simultaneous J- and H-band observations using MIRC-X, the first of their kind. This data is complemented with observations in the K-band from the "CLassic Interferometry with Multiple Baselines" (CLIMB) beam combiner. The observations are introduced in Section . Our modelling techniques and temperature gradient analysis are shown in Section REF . The details of our companion search are outlined in Section REF  and we discuss the implications and draw conclusions in Sections  and , respectively.
